An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.
George Mason University (USA) -
University of Michigan (USA) -
University of Cambridge (UK)
CHIANTI consists of a critically evaluated set of up-to-date atomic
data, together with user-friendly programs written
in Interactive Data Language (IDL) and Python to calculate the spectra
from astrophysical plasmas.
The CHIANTI package is freely available.
If you use the package, we only ask you to
acknowledge CHIANTI .
- The Chianti wine-producing area of Tuscany, Italy -
CHIANTI Database Version 7.1.4 released on May 20, 2014
The splups file for Fe XXI, which included the electron impact effective
collision strengths, was inadvertently missing some data for collisional
excitation from levels 4 and 5 of the ground configuration to higher levels.
This omission caused level populations for these two levels to be inaccurate at densities above about 10^13 cm^-3.
The A-values for the O II 1-5 transition 2s2.2p3 4S1.5-2s2.2p3 2P1.5 at 2471.09A and the 1-4 2s2.2p3 4S1.5-2s2.2p3 2P0.5 at 2470.97A were found to be reversed.
The file containing the parameters for dielectronic recombination for Al II,
al_2.drparams, had become corrupted. The file has been repaired and a new
ionization balance file has been calculated. The error mainly affected the
ionization balance of Al I and Al II.
CHIANTI Version 7.1 released
The main feature of CHIANTI Version 7.1 is the inclusion of a large
number of configurations to the atomic models of Fe VIII to XIV. These
configurations give rise to a forest of spectral lines in the 50-170 A
wavelength range that contribute significantly to the total radiative
output of the Sun at those wavelengths. Also, they give rise to several
strong lines that are currently neglected by spectral codes, and provide
significant contributions to the SDO/AIA bandpasses centered at 94A
and 131A. These data are calculated using the Flexible Atomic Code
(FAC) under the distorted wave approximation.
Additional data for a few more ions are included, that improve
the available datasets for a few ions, and correct a few glitches for
other ions at all wavelength ranges. New element abundance data
sets are provided, and improved recombination rates are included
and used to provide a new set of CHIANTI ionization equilibria
We are grateful to
individual scientists and funding agencies for their support.